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We present the first numerical simulations in coupled dark energy cosmologieswith high enough resolution to investigate the effects of the coupling ongalactic and sub-galactic scales. We choose two constant couplings and atime-varying coupling function and we run simulations of three Milky-Way-sizehalos ($\sim$10$^{12}$M$_{\odot}$), a lower mass halo(6$\times$10$^{11}$M$_{\odot}$) and a dwarf galaxy halo(5$\times$10$^{9}$M$_{\odot}$). We resolve each halo with several millions darkmatter particles. On all scales the coupling causes lower halo concentrationsand a reduced number of substructures with respect to LCDM. We show that thereduced concentrations are not due to different formation times, but they arerelated to the extra terms that appear in the equations describing thegravitational dynamics. On the scale of the Milky Way satellites, we show thatthe lower concentrations can help in reconciling observed and simulatedrotation curves, but the coupling values necessary to have a significantdifference from LCDM are outside the current observational constraints. On theother hand, if other modifications to the standard model allowing a highercoupling (e.g. massive neutrinos) are considered, coupled dark energy canbecome an interesting scenario to alleviate the small-scale issues of the LCDMmodel.

Effects of Coupled Dark Energy on the Milky Way and its Satellites